The Evolving Effect of Cosmic Web Environment on Galaxy Quenching

Hasan, Farhanul; Burchett, Joseph N.; Abeyta, Alyssa; Hellinger, Douglas; Mandelker, Nir; Primack, Joel R.; Faber, S. M.; Koo, David C.; Elek, Oskár; Nagai, Daisuke

doi:10.3847/1538-4357/acd11c

Cited by 8 publications

(3 citation statements)

References 108 publications

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“…Such dependence on the connectivity of the cosmic web suggests that it has crucial roles in providing the main source of fuel for galaxy growth. An analysis of the IllustrisTNG simulation [119] by [120] finds significant dependence of galaxy properties on the cosmic web environment. They show that the cosmic web structures efficiently channel cold gas into most galaxies leading to such dependence.…”

Section: Discussionmentioning

confidence: 99%

The correlations between galaxy properties in different environments of the cosmic web

Nandi,

Pandey,

Sarkar

2024

J. Cosmol. Astropart. Phys.

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We study the correlations between (u-r) colour, stellar mass, specific star formation rate (sSFR) and metallicity of galaxies in different geometric environments of the cosmic web using a volume limited sample from the SDSS. The geometric environment at the location of each galaxy is determined using the eigenvalues of the tidal tensor in three dimensions. We use the Pearson correlation coefficient (PCC) and the normalized mutual information (NMI) to quantify the correlations between these galaxy properties in sheets, filaments and clusters after matching the stellar mass distributions of the galaxies in these environments. A two-tailed t-test assesses the statistical significance of the observed differences between these relations in different geometric environments. The null hypothesis can be rejected at >99.99% significance level in most of the cases, suggesting that the scaling relations between the observable galaxy properties are susceptible to the geometric environments of the cosmic web.

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Section: Discussionmentioning

confidence: 99%

The correlations between galaxy properties in different environments of the cosmic web

Nandi,

Pandey,

Sarkar

2024

J. Cosmol. Astropart. Phys.

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“…Recent advances in cosmic web reconstruction techniques have enabled us to study the impact of filaments on various aspects of galaxy formation. These studies have explored the effect of filaments on quenching (e.g., Kuutma et al 2017;Laigle et al 2018;Xu et al 2020;Winkel et al 2021;Hasan et al 2023;Bulichi et al 2024), gas supply (e.g., Stark et al 2016;Kleiner et al 2017;Crone Odekon et al 2018;Song et al 2021;Galárraga-Espinosa et al 2022;Rosas-Guevara et al 2022;Zhu et al 2022), and alignment between galaxy spin and filament direction (e.g., Dubois et al 2014;Codis et al 2018;Ganeshaiah Veena et al 2019;Kraljic et al 2019;Pandya et al 2019;Blue Bird et al 2020;Welker et al 2020;Tudorache et al 2022), in both observations and simulations. However, the methods used to identify filaments vary widely, and the conclusions drawn regarding the physical effect of filaments on galaxy formation phenomena are often divergent.…”

Section: Introductionmentioning

confidence: 99%

“…However, the methods used to identify filaments vary widely, and the conclusions drawn regarding the physical effect of filaments on galaxy formation phenomena are often divergent. For example, while some studies suggest a suppression of gas (e.g., Crone Odekon et al 2018;Zhu et al 2022;Hasan et al 2023) and star formation (e.g., Alpaslan et al 2016;Kraljic et al 2018;Malavasi et al 2022) near filaments, others report an increase in gas supply and/or star formation (e.g., Kleiner et al 2017;Vulcani et al 2019;Kotecha et al 2022).…”

Section: Introductionmentioning

confidence: 99%

Filaments of the Slime Mold Cosmic Web and How They Affect Galaxy Evolution

Hasan,

Burchett,

Hellinger

et al. 2024

ApJ

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We present a novel approach for identifying cosmic web filaments within the DisPerSE structure identification framework, using cosmic density field estimates from the Monte Carlo Physarum Machine (MCPM), inspired by the slime mold organism. We apply our method to the IllustrisTNG (TNG100) cosmological simulations and investigate the impact of filaments on galaxies. The MCPM density field is superior to the Delaunay tessellation field estimator in tracing the true underlying matter distribution and allows filaments to be identified with higher fidelity, finding more low-prominence/diffuse filaments. Using our new filament catalogs, we find that ≳90% of galaxies are located within ∼1.5 Mpc of a filamentary spine, with little change in the median star formation activity with distance to the nearest filament. Instead, we uncover a differential effect of the local filament line density, Σfil (MCPM)—the total MCPM overdensity per unit length along a filament segment—on galaxy formation: most galaxies are quenched and gas-poor near high-line density filaments at z ≤ 1. At earlier times, the filamentary environment appears to have no effect on galactic gas supply and quenching. At z = 0, quenching in log ( M * / M ⊙ ) ≳ 10.5 galaxies is mainly driven by mass, while lower-mass galaxies are significantly affected by the filament line density. Satellites are far more susceptible to filaments than centrals. The local environments of massive halos are not sufficient to account for the effect of filament line density on gas removal and quenching. Our new approach holds great promise for observationally identifying filaments from galaxy surveys such as SDSS and DESI.

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The relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

Mountrichas

Yang

Buat

et al. 2023

A&A

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In this work, we study the relation of the cosmic environment and morphology with the star formation and stellar population of galaxies. Most importantly, we examine if this relation differs for systems with active and non-active supermassive black holes. For that purpose, we used 551 X-ray detected active galactic nuclei (AGNs) and 16 917 non-AGN galaxies in the COSMOS-Legacy survey for which surface-density field measurements are available. The sources lie at a redshift of 0.3 < z < 1.2, probe X-ray luminosities of 42 < log[LX,2−10 keV(erg s−1)] < 44, and have stellar masses of 10.5 < log [M*(M⊙)] < 11.5. Our results show that isolated AGNs (field) have lower star formation rates (SFRs) compared to non-AGNs at all LX spanned by our sample. However, in denser environments (filaments and clusters), moderate LX AGN (log[LX,2−10 keV(erg s−1)] > 43) and non-AGN galaxies have similar SFRs. We also examined the stellar populations and the morphology of the sources in different cosmic fields. For the same morphological type, we find that non-AGN galaxies tend to have older stellar populations and are less likely to have undergone a recent burst in denser environments compared to their field counterparts. The differences in the stellar populations concerning density field are mainly driven by quiescent systems. Moreover, low LX AGNs present negligible variations of their stellar populations in all cosmic environments, whereas moderate LX AGNs have, on average, younger stellar populations and are more likely to have undergone a recent burst in high-density fields. Finally, in the case of non-AGN galaxies, the fraction of bulge-dominated (BD) systems increases with the density field, while BD AGNs are scarce in denser environments. Our results are consistent with a scenario in which a common mechanism, such as mergers, triggers both the star-formation and the AGN activity.

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The Evolving Effect of Cosmic Web Environment on Galaxy Quenching

Cited by 8 publications

References 108 publications

The correlations between galaxy properties in different environments of the cosmic web

The correlations between galaxy properties in different environments of the cosmic web

Filaments of the Slime Mold Cosmic Web and How They Affect Galaxy Evolution

The relation of cosmic environment and morphology with the star formation and stellar populations of AGN and non-AGN galaxies

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